More recently, the CARMENES spectrograph and consortium (introduced in Sect. REF ) has been responsible for increasing the number of detected planets around M dwarfs in binary systems, particularly around wide separation systems, namely, HD 180617 [1]}, Gl 49 [2]}, LTT 3780 [3]}, [4]}, HD 79211 [5]}, GJ 3473 [6]}, and HD 238090 [7]}.
Precise stellar properties, as well as radial velocities (RVs), are commonly determined solely for the host; the details of the companion are often missed, with some exceptions, such as GJ 338 B [5]} or GJ 15 A and B [9]}, [10]}, [11]}. Studying properties such as metallicity and age can shed light on which environments favor the formation of particular planets [12]}, [13]}, [14]}. Observing more systems would allow for a better grasp on how stellar multiplicity in M-dwarf systems plays a role in the planet formation process and in the types of planets that can exist.
